A complication is that in reality, the accretion history, not only the instantaneous values, likely sets the radius. This is suggested by the results of [1]}, who find that during formation, planets can have a radiative (and not convective) structure for a large fraction of their outer mass layers. Thus the results of classical convective-planet structures that let us write \(R_{\mathrm {p}}=R_{\mathrm {p}}(\dot{M},M_{\mathrm {p}})\) , with no time dependence, might be a simplification. However, we effectively mitigate this by considering the two different fits (“cold” and “hot”), and will find that the radius does not have a major influence in any case.
